Search results
Results From The WOW.Com Content Network
Cepheid variables are divided into two subclasses which exhibit markedly different masses, ages, and evolutionary histories: classical Cepheids and type II Cepheids. Delta Scuti variables are A-type stars on or near the main sequence at the lower end of the instability strip and were originally referred to as dwarf Cepheids.
[citation needed] The rate of change of the period of a Cepheid variable, along with chemical abundances detectable in the spectrum, can be used to deduce which crossing a particular star is making. [15] Classical Cepheid variables were B type main-sequence stars earlier than about B7, possibly late O stars, before they ran out of hydrogen in ...
The following is a list of variable stars that are well-known, bright, ... Classical Cepheid (DCEP) R Aql: Aquila 5 m.5 12 m.0 6.5: 284 d Mira variable (M)
In astronomy, a period-luminosity relation is a relationship linking the luminosity of pulsating variable stars with their pulsation period. The best-known relation is the direct proportionality law holding for Classical Cepheid variables, sometimes called the Leavitt Law.
A variable star is a star whose brightness as seen from Earth (its apparent magnitude) ... the first known representative of the class of Cepheid variables.
Type II Cepheids are not as well known as their type I counterparts, with only a couple of naked eye examples. In this list, the period quoted for RV Tauri variables is the interval between successive deep minima, hence twice the comparable period for the other sub-types.
η Aquilae A is a Cepheid variable star, discovered by Edward Pigott in 1784. [ 14 ] [ 3 ] It has an apparent magnitude that ranges from 3.49 to 4.3 over a period of 7.177 days. [ 3 ] Along with Delta Cephei , Zeta Geminorum and Beta Doradus , it is one of the most prominent naked eye Cepheids; [ 15 ] that is, both the star itself and the ...
The constellation's brightest star is Alderamin (Alpha Cephei), with an apparent magnitude of 2.5. Delta Cephei is the prototype of an important class of star known as a Cepheid variable. RW Cephei, an orange hypergiant, together with the red supergiants Mu Cephei, MY Cephei, VV Cephei, V381 Cephei, and V354 Cephei are among the largest stars ...